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Table 3

Summary of the samples and data used in this paper.

Sample Number of galaxies used here Relevant references Optical spectra H I masses Metallicity indicator min log M (M) max log M (M) Notes
(1) (2) (3) (4) (5) (6) (7) (8) (9)
H IX 10 Lutz et al. (2017, 2018) Y Y PP04 O3N2, N2 9.8 10.6

IC 4857 1 As H IX Y Y PP04 O3N2, N2 10.5 Member of the original CONTROL sample

HIPASS 1796 Dénes et al. (2014); Barnes et al. (2001); Meyer et al. (2004); Doyle et al. (2005) N Y 8.0 11.5 Biased towards H I-rich objects, maximal redshift 0.04, parent sample for H IX galaxies

SDSS MPA-JHU 60021 Abazajian et al. (2009); Salim et al. (2007) Y N PP04 O3N2 8.0 11.5 To provide a benchmark mass-metallicity relation

GASS with longslit spectroscopy 96 Catinella et al. (2018); Moran et al. (2012) Y Y PP04 O3N2 10.0 10.82 Longslit spectra typically out to 1 Petrosian 90% radius, see text for sample selection

CALIFA 227 Sánchez et al. (2014) Y N PP04 O3N2 9.0 11.2 IFU data, the metallicity gradient is typically measured between 0.5 and 2 effective radii

Notes. Column (1): name of the sample. Column (2): number of galaxies used in this paper. Column (3): references to the papers in which the sample and/or data are described in more detail. Column (4): whether (Y) or not (N) optical spectra are available for this sample. Column (5): whether (Y) or not (N) measurements of the H I mass are available for this sample. Column(6): which metallicity indicator was used to estimate the gas-phase metallicity. PP04 refers to Pettini & Pagel (2004). Columns (7) and (8): minimum and maximum stellar mass limit of the sample, respectively. Column (9): further notes.

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